The residuals for the remaining three spectra are compared graphically
in Fig. REF  and listed numerically in
Table REF . Residuals that differ from zero by more
than \(2 \sigma \)  assuming that the cosmology and foreground model
are known exactly are marked in red in Table
REF . The three spectra are in very good
agreement. The nearly \(\sim 2\sigma \)  upward fluctuation at \(\ell _b\approx 489\)  and \(\sim 2.5\sigma \)  downward fluctuation at \(\ell _b =794\)  (which have been noted by some theorists e.g. [1]})
are reproduced in all of the Planck spectra and are clearly real
features of the primordial CMB spectrum. The general oscillatory
patterns in the residuals, which various authors (e.g. [2]}) have claimed might be related to an
inconsistency in the lensing smoothing of the acoustic peaks (and
related to the high value of \(A_L\)  measured from Planck TT, see
Fig. REF ) are also reproduced
across the three spectra (see also Fig. 12 of [3]}). The most deviant point in
Fig. REF  is for the \(217 \times 217\) 
spectrum in the band centred at \(\ell = 1469\)  (as noted in
PPL15 and PCP18). This band power deviates from zero by \(2.63 \sigma \)  on the
assumption that the cosmology and foreground model is known exactly
(which is, of course, not true).
